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The Average Star Formation Histories of Galaxies in Dark Matter Halos from z = 0-8
We present a robust method to constrain average galaxy star formation rates (SFRs), star formation histories (SFHs), and the intracluster light (ICL) as a function of halo mass. Our results are
Star Formation in AEGIS Field Galaxies since z = 1.1: The Dominance of Gradually Declining Star Formation, and the Main Sequence of Star-forming Galaxies
We analyze star formation (SF) as a function of stellar mass (M☉) and redshift z in the All-Wavelength Extended Groth Strip International Survey. For 2905 field galaxies, complete to 10^10(10^10.8 )M
The Universal Stellar Mass-Stellar Metallicity Relation for Dwarf Galaxies
We present spectroscopic metallicities of individual stars in seven gas-rich dwarf irregular galaxies (dIrrs), and we show that dIrrs obey the same mass-metallicity relation as the dwarf spheroidal
HYPERACCRETING BLACK HOLES AND GAMMA-RAY BURSTS
A variety of current models of gamma-ray bursts (GRBs) suggest a common engine: a black hole of several solar masses accreting matter from a disk at a rate of 0.01 to 10 M☉ s-1. Using a numerical
Multi-element Abundance Measurements from Medium-resolution Spectra. III. Metallicity Distributions of Milky Way Dwarf Satellite Galaxies
We present metallicity distribution functions (MDFs) for the central regions of eight dwarf satellite galaxies of the Milky Way: Fornax, Leo I and II, Sculptor, Sextans, Draco, Canes Venatici I, and
Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure
We use the "Via Lactea" simulation to study the co-evolution of a Milky Way-sized ΛCDM halo and its subhalo population. While most of the host halo mass is accreted over the first 6 Gyr in a series
Dark Matter Substructure and Gamma-Ray Annihilation in the Milky Way Halo
We present initial results from Via Lactea, the highest resolution simulation to date of Galactic CDM substructure. It follows the formation of a Milky Way-sized halo with Mhalo = 1.8 ? 1012 M? in a
The Major and Minor Galaxy Merger Rates at z < 1.5
Calculating the galaxy merger rate requires both a census of galaxies identified as merger candidates, and a cosmologically-averaged‘observability’ timescale hTobs(z)ifor identifying galaxy mergers.
The M31 Velocity Vector. II. Radial Orbit toward the Milky Way and Implied Local Group Mass
We determine the velocity vector of M31 with respect to the Milky Way and use this to constrain the mass of the Local Group, based on Hubble Space Telescope proper-motion measurements of three fields
On the Lack of Evolution in Galaxy Star Formation Efficiency
Using reconstructed galaxy star formation histories, we calculate the instantaneous efficiency of galaxy star formation (i.e., the star formation rate divided by the baryon accretion rate) from z = 8
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